DIURNAL VARIATIONS IN THE NUMBER OF SHOWER METEORS DETECTED BY THE FORWARD-SCATTERING OF RADIO WAVES: PART III. ELLIPSOIDAL THEORY

1958 ◽  
Vol 36 (1) ◽  
pp. 117-126 ◽  
Author(s):  
C. O. Hines
Keyword(s):  
Forward Scattering ◽  
Diurnal Variations ◽  
New Method ◽  
Radio Waves ◽  
Meteor Showers ◽  
Rigorous Results ◽  
Forward Scatter ◽  
Scatter Process ◽  
Full Development

A theory of meteor 'observability' relating to forward-scatter radio experiments was developed in Part I of this series, with the use of a simplifying 'cylindrical approximation'. The application of the theory to data obtained during meteor showers provides a promising new method for studying the intrinsic strengths of the showers. The principal limitation of the method is due to the inaccuracies of the cylindrical approximation. In the present paper, these inaccuracies are removed by a full development of the ellipsoidal geometry inherent in the forward-scatter process. The more rigorous results are compared with the approximate results at various stages throughout the analysis.

DIURNAL VARIATIONS IN THE NUMBER OF SHOWER METEORS DETECTED BY THE FORWARD-SCATTERING OF RADIO WAVES: PART II. EXPERIMENT

1955 ◽  
Vol 33 (10) ◽  
pp. 600-606 ◽  
Author(s):  
P. A. Forsyth ◽  
C. O. Hines ◽  
E. L. Vogan
Keyword(s):  
Specular Reflection ◽  
Forward Scattering ◽  
Diurnal Variations ◽  
Radio Waves ◽  
Forward Scatter ◽  
Transmission Path ◽  
Signal Rate ◽  
Cedar Rapids ◽  
Good Agreement

The theory developed in Part I is applied to derive the expected diurnal variations of the meteor signal rate for four showers as observed by means of a particular forward-scatter transmission path (Cedar Rapids – Ottawa). These results are then compared with the experimental signal rates. The good agreement obtained indicates that the approximations inherent in the theory are sufficiently accurate for practical purposes. The results also indicate that very few meteors, if any, are observed under conditions which do not satisfy the requirements for specular reflection.

DIURNAL VARIATIONS IN THE NUMBER OF SHOWER METEORS DETECTED BY THE FORWARD-SCATTERING OF RADIO WAVES: PART I. THEORY

1955 ◽  
Vol 33 (9) ◽  
pp. 493-503 ◽  
Author(s):  
C. O. Hines
Keyword(s):  
Diurnal Variation ◽  
Incidence Rate ◽  
Forward Scattering ◽  
Diurnal Variations ◽  
Time Interval ◽  
Weight Factor ◽  
Radio Waves ◽  
Meteor Trails

Various observational factors affect the number of shower meteors which can be detected, in a given time interval, by the scattering of radio waves from the ionized meteor trails. The pertinent factors in the case of forward-scattering, where the transmitter and receiver are widely separated, are expressed approximately as functions of the position of the shower radiant. In combination, they provide an observational weight factor which may change appreciably as the radiant moves in the course of a day. The consequent diurnal variation in the occurrence of scattered signals may then be determined, and distinguished from variations due to random changes in the incidence rate of the meteors.

scholarly journals 58. Results of observations of the scattering of radio waves by the electronic inhomogeneities of the solar corona

1957 ◽  
Vol 4 ◽  
pp. 313-317
Author(s):  
V. V. Vitkevitch
Keyword(s):  
Solar Corona ◽  
Radio Source ◽  
Crab Nebula ◽  
New Method ◽  
Radio Waves ◽  
The Crab Nebula

A new method for the investigation of the solar corona, suggested by us (Vitkevitch, 1951) [1], consists of observing the radio source identified with the Crab nebula (NGC 1952; α = 05h 31m 40s, δ = 22° 10′) when it is covered by the solar corona. This occurs every year on 14–15 June.

Ionization profile of meteors from simultaneous video and radio forward scatter observations

2020 ◽  
Author(s):  
Hervé Lamy ◽  
Michel Anciaux ◽  
Sylvain Ranvier ◽  
Antoine Calegaro ◽  
Carl Johannink
Keyword(s):  
Peak Power ◽  
Specular Reflection ◽  
Radio Waves ◽  
Line Density ◽  
Science And Engineering ◽  
Forward Scatter ◽  
Electron Line ◽  
Power Profile ◽  
Video Observations ◽  
Polarization Factor

<p>In this study, optical video observations of meteors with the CAMS (Camera for All-sky Meteor Surveillance)-BeNeLux network and radio forward scatter observations with the BRAMS (Belgian RAdio Meteor Stations) network obtained on 4-5 October 2018  are combined in order to obtain an ionization profile along a meteor path.</p><p>The trajectory, initial speed and deceleration parameters of a given meteor are provided by the CAMS-BeNeLux data. For a given trajectory, the positions of the specular reflection points for radio waves are computed for each combination of a given BRAMS receiving station and the BRAMS transmitter. For each receiving station which recorded a meteor echo (depending on the geometry and the SNR ratio), the power profile is computed and the peak power values of the underdense meteor profiles are used to determine the ionization (electron line density) at the various specular reflection points along the meteor path. This is done using the McKinley (1961) formula which is strictly valid for underdense meteor echoes.  We discuss how we compute the gains of the antennas, the polarization factor, and how the peak power values are transformed from arbitrary units into watts using the signal recorded from a device called the BRAMS calibrator. We also discuss how to extend this study to overdense meteor echoes or those with intermediate electron line densities.</p><p>Finally, these results are combined with a simple ablation meteor model in order to obtain an estimate of the initial mass of the meteoroid.</p><p>Mc Kinley D.W.R., Meteor science and engineering, Mc Graw-Hill eds, 1961</p>

scholarly journals The Birth and Evolution of Stanislavsky’s Method

2017 ◽  
Vol 7 (1) ◽  
pp. 299-305
Author(s):  
Daniela Cojan
Keyword(s):  
Creative Process ◽  
New Method ◽  
Important Lesson ◽  
Full Development ◽  
Body And Soul

Abstract The stanislavskian system arises in full development of the realist current. Starting from the word, the actor expresses through gestures, intonations and mimics. The pre-stanislavskian actor is dominated by dilentatism and emotional “accidents”, the balance is tilted to an act full of clichés and crafts. Perhaps the most important lesson that Stanislavsky gives us is that for the actor in his work to reach a credible character, he must go through all states, sensations and feelings required in building a character. We cannot forget, however, that Stanislavsky devised a new method of representation also due to the emergence of Chekhovian texts. To give effect to the new ways of writing, the attention must focus on the actors, without neglecting the scenography. Stanislavsky wants to convince the actor that if he doesn’t want to use tricks to present truth, he should be just like a painter or musician, to devote his whole being, “body and soul especially” in the creative process.

MONITORING OF COASTAL ECOSYSTEMS BY METHOD OF REMOTE SENSING IN THE SHORT-WAVE RANGE OF RADIO WAVES

2017 ◽  
Author(s):  
Sergej Belov ◽  
Sergej Belov ◽  
Ija Belova ◽  
Ija Belova ◽  
Stepan Falomeev ◽  
...  
Keyword(s):  
Remote Sensing ◽  
Comparative Analysis ◽  
Short Wave ◽  
Coastal Ecosystems ◽  
Relative Accuracy ◽  
New Method ◽  
Radio Waves ◽  
Signal Noise ◽  
Order Of Magnitude ◽  
Wave Range

A new method for estimating the parameter noncoherent signal/noise K of ionospheric signal is offered. A comparative analysis is carrying out. This new method exceeds an order of magnitude widely used standard one by analytical (relative) accuracy of determining a parameter K. It has the same order as the well-known coherent methodology.

THE FORWARD-SCATTERING OF RADIO WAVES FROM OVERDENSE METEOR TRAILS

1957 ◽  
Vol 35 (9) ◽  
pp. 1033-1041 ◽  
Author(s):  
C. O. Hines ◽  
P. A. Forsyth
Keyword(s):  
Charge Density ◽  
Forward Scattering ◽  
Point Of View ◽  
Radio Waves ◽  
Geometric Factors ◽  
Meteor Trails

The forward-scattering of radio waves from overdense meteor trails is treated from an elementary point of view. The results indicate that the same geometric factors enter this problem as enter the problem of forward-scattering from underdense trails, and that the transition between underdense and overdense trails occurs at the same value of charge density as in the backscatter case. These conclusions are not expected to be generally valid when applied to individual trails, but at least they should provide a valid basis for the interpretation and prediction of the effects produced statistically by a large number of trails.

THE NUMBER DENSITY OF METEOR TRAILS OBSERVABLE BY THE FORWARD-SCATTERING OF RADIO WAVES

1956 ◽  
Vol 34 (10) ◽  
pp. 997-1004 ◽  
Author(s):  
Robert E. Pugh
Keyword(s):  
Forward Scattering ◽  
Radio Waves ◽  
Number Density ◽  
Meteor Trails

The number of meteor trails which can be detected by the forward-scattering of radio waves varies with the region of the sky under observation. The number density is determined theoretically, as a function of position relative to the transmitter and receiver.

A THEORETICAL RATE–AMPLITUDE RELATION IN METEORIC FORWARD-SCATTERING

1958 ◽  
Vol 36 (5) ◽  
pp. 539-554 ◽  
Author(s):  
C. O. Hines
Keyword(s):  
Observational Data ◽  
Forward Scattering ◽  
Occurrence Rate ◽  
Radio Waves ◽  
Scaling Factors ◽  
Meteor Trails ◽  
Amplitude Level ◽  
Good Agreement

The theory of the forward-scattering of radio waves by ionized meteor trails is applied to the development of a rate-amplitude relation. This relation expresses the anticipated occurrence rate of scattered signals which exceed a chosen amplitude level, as a function of that level. It is compared with preliminary observational data, and found to be in good agreement both qualitatively and quantitatively. Closest agreement is obtained only with an appropriate choice of two scaling factors. These provide an abstract of the observations in a form which is convenient for further study and interpretation.

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